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Multi-field Mimetic Gravity

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arxiv 2108.11666 v3 pith:LTR2AD3A submitted 2021-08-26 gr-qc astro-ph.COhep-th

classification gr-qcastro-ph.COhep-th
keywords backgroundfieldmimeticmulti-fieldperturbationspacetrajectorycurved
verification ladder T0 review T1 audit T2 compute T3 formal
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In this paper, we extend the mimetic gravity to the multi-field setup with a curved field space manifold. The multi-field mimetic scenario is realized via the singular limit of the conformal transformation between the auxiliary and the physical metrics. We look for the cosmological implications of the setup where it is shown that at the background level the mimetic energy density mimics the roles of dark matter. At the perturbation level, the scalar field perturbations are decomposed into the tangential and normal components with respect to the background field space trajectory. The adiabatic perturbation tangential to the background trajectory is frozen while the entropy mode perpendicular to the background trajectory propagates with the speed of unity. Whether or not the entropy perturbation is healthy directly depends on the signature of the field-space metric. We perform the full non-linear Hamiltonian analysis of the system with the curved field space manifold and calculate the physical degrees of freedom verifying that the system is free from the Ostrogradsky-type ghost.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Quantum cosmological perturbations in bouncing models with mimetic dark matter

    astro-ph.CO 2025-06 conditional novelty 6.0 of 10

    Mimetic dark matter bouncing cosmologies can generate scale-invariant, slightly red-tilted primordial fluctuations matching CMB observations when the bounce scale lies between 10^5 and 10^9 Planck lengths.

  2. New generalization of the Barboza-Alcaniz parametrization of Dark energy

    gr-qc 2026-07 reject novelty 4.0 of 10

    A generalized Barboza-Alcaniz dark-energy parametrization with a free exponent n is fit to cosmological data, but the model analyzed does not actually resolve the future-time problem it was designed to fix.

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